Planetary Motions and Lessons in Science

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# Planetary Motions and Lessons in Science - PowerPoint PPT Presentation

Planetary Motions and Lessons in Science . Can One Prove that the Earth is Round?. Height of Polaris above the horizon. Shadow of the Earth during a lunar eclipse. Can One Prove that the Earth is Round?. Eratosthenes experiment. Height of Polaris above the horizon.

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Presentation Transcript

Planetary Motions

and

Lessons in Science

Can One Prove that the Earth is Round?
• Height of Polaris above the horizon
• Shadow of the Earth during a lunar eclipse
Can One Prove that the Earth is Round?
• Eratosthenes experiment
• Height of Polaris above the horizon
• Shadow of the Earth during a lunar eclipse

Inferred size of Earth: 250,000 stadia

This is either 20% off, or good to about 1%, depending on the definition of stadia.

Can One Prove that the Earth goes Around the Sun?

Proof of motion is throughparallax

An object’s position will appear to shift due to change in the observer’s position.

This MUST occur!!!

Since parallax was not seen, the Earth must not be moving!

Geocentric Properties of the Original Planets(Mercury, Venus, Mars, Jupiter, Saturn)
• The word “planet” means “wanderer”.
• The planets always stay close to the ecliptic plane, i.e., they move through the zodiac constellations.
• Mercury and Venus areinferior planets– they are never seen very far from the Sun (Mercury never more 23°, Venus never more than 46°).
• Mars, Jupiter, and Saturn aresuperior planets, and can be found anywhere in the zodiac.
• Planets usuallymove west-to-east against the fixed stars. But sometimes the planets move backwards (east-to-west). This is called retrograde motion.

Path of a planet with respect to the background stars

Path of a planet with respect to the background stars

The Science of Aristotle
• Aristotle’s ideas:
• Heavy objects fall faster than light objects
• Objects have inertia – all objects prefer to be at rest
• The heavens are perfect and immutable
• All heavenly objects travel about the Earth at a constant speed in a perfect circle

So how did Aristotle explain retrograde motion?

Explaining Retrograde Motion:Aristotle’s Model (350 B.C.)
• Earth at the center (since it is not moving).
• Sun and Moon orbit the Earth (west to east).
• Planets move at a constant speed around small circles calledepicycles.
• Epicycles orbit around Earth (west-to-east) at a constant speed in a circle called a deferent.

Combination of orbital and epicyclic motion creates retrograde motion.

Explaining Retrograde Motion:Aristotle’s Model (350 B.C.)
• Earth at the center (since it is not moving).
• Sun and Moon orbit the Earth (west to east).
• Planets move at a constant speed around small circles calledepicycles.
• Epicycles orbit around Earth (west-to-east) at a constant speed in a circle called a deferent.

Combination of orbital and epicyclic motion creates retrograde motion.

Trouble is, it doesn’t do a very good job of predicting exact positions.

• Put the Earth slightly off center at a point called theeccentric
• State that epicycles only move at a constant speed about the deferent when viewed from a special place called theequant

Model is more complicated, and, though it does better, it still doesn’t predict the exact positions of the planets.

Since the planets are in the heavens, they must move in perfect circles at a constant speed. But …

• The heavenly bodies do not all move around the same center.
• The Earth is not at the center of the planetary system (i.e., the universe). Only the Moon goes around the Earth.
• The Sun is at the center of the planetary system.
• Compared to the distance of the fixed stars, the distance from the Earth to the Sun is negligible.
• The daily revolution of the sky is due to the Earth’s rotation.
• The Sun’s annual motion is due to the Earth’s orbit around the Sun.
• Retrograde motion is due to the Earth’s orbit around the Sun.

Retrograde motion is explained by the Earth “passing” (or being passed by) another planet in its orbit.

Retrograde motion is explained by the Earth “passing” (or being passed by) another planet in its orbit.

The Heliocentric Model

The Heliocentric model also naturally explains the difference between inferior and superior planets.

But the model is no better at predicting the positions of the planets than Aristotle’s model. (And are the stars really so far away that we can’t see parallax???)

Galileo’s Experiments

Galileo tried something new – doing experiments!

• Dropping balls to measure gravity
• Rolling balls to examine inertia
• Observing the sky through a telescope!
What Galileo Saw
• An imperfect Sun (sunspots)
What Galileo Saw
• An imperfect Sun (sunspots)
• A Moon with mountains and craters
What Galileo Saw
• An imperfect Sun (sunspots)
• A Moon with mountains and craters
• The “ears” of Saturn
What Galileo Saw
• An imperfect Sun (sunspots)
• A Moon with mountains and craters
• The “ears” of Saturn
• Four moons orbiting Jupiter
What Galileo Saw
• An imperfect Sun (sunspots)
• A Moon with mountains and craters
• The “ears” of Saturn
• Four moons orbiting Jupiter
• The Milky Way’s stars
What Galileo Saw
• An imperfect Sun (sunspots)
• A Moon with mountains and craters
• The “ears” of Saturn
• Four moons orbiting Jupiter
• The Milky Way’s stars
• The Phases of Venus